Dynamical evolution of the Cybele asteroids

  title={Dynamical evolution of the Cybele asteroids},
  author={Valerio Carruba and David Nesvorn'y and Safwan Aljbaae and M. E. Huaman},
  journal={Monthly Notices of the Royal Astronomical Society},
The Cybele region, located between the 2J:-1A and 5J:-3A mean-motion resonances, is adjacent and exterior to the asteroid main belt. An increasing density of three-body resonances makes the region between the Cybele and Hilda populations dynamically unstable, so that the Cybele zone could be considered the last outpost of an extended main belt. The presence of binary asteroids with large primaries and small secondaries suggested that asteroid families should be found in this region, but only… Expand
On the oldest asteroid families in the main belt
Asteroid families are groups of minor bodies produced by high-velocity collisions. After the initial dispersions of the parent bodies fragments, their orbits evolve because of several gravitationalExpand
The Karin cluster is a young asteroid family thought to have formed only $\simeq 5.75$~My ago. The young age can be demonstrated by numerically integrating the orbits of Karin cluster membersExpand
Influence of the Centaurs and TNOs on the main belt and its families
Centaurs are objects whose orbits are found between those of the giant planets. They are supposed to originate mainly from the Trans-Neptunian objects, and they are among the sources of Near-EarthExpand
The Hoffmeister asteroid family
The Hoffmeister family is a C-type group located in the central main belt. Dynamically, it is important because of its interaction with the ${\nu}_{1C}$ nodal secular resonance with Ceres, thatExpand
On the highly inclined vW leptokurtic asteroid families
$v_W$ leptokurtic asteroid families are families for which the distribution of the normal component of the terminal ejection velocity field $v_W$ is characterized by a positive value of theExpand
On the Astrid asteroid family
Among asteroid families, the Astrid family is peculiar because of its unusual inclination distribution. Objects at $a\simeq$~2.764 au are quite dispersed in this orbital element, giving the family aExpand
Ancient and primordial collisional families as the main sources of X-type asteroids of the inner main belt
Aims. The near-Earth asteroid population suggests the existence of an inner main belt source of asteroids that belongs to the spectroscopic X complex and has moderate albedos. The identification ofExpand
Footprints of a possible Ceres asteroid paleo-family
Ceres is the largest and most massive body in the asteroid main belt. Observational data from the Dawn spacecraft reveal the presence of at least two impact craters about 280~km in diameter on theExpand
Yarkovsky V-shape identification of asteroid families
Abstract There are only a few known main belt (MB) asteroid families with ages greater than 2  Gyr (Brož et al., 2013; Spoto et al., 2015). Estimates based on the family producing collision rateExpand
On the age of the Beagle secondary asteroid family
Abstract The Beagle family is a C-type subgroup of the Themis family, in the outer main belt. Previous works suggested that it could be younger than 20 Myr and a possible source for the dust in the iExpand


The stable archipelago in the region of the Pallas and Hansa dynamical families
Among highly inclined asteroids, the region of the central main belt between the 3J:–1A and 5J:–2A mean-motion resonances has long been known to host the Pallas and Hansa dynamical families. ThisExpand
Constraining the cometary flux through the asteroid belt during the late heavy bombardment
In the Nice model, the late heavy bombardment (LHB) is related to an orbital instability of giant planets which causes a fast dynamical dispersion of a transneptunian cometary disk. We study effectsExpand
The peculiar case of the Agnia asteroid family
The Agnia asteroid family, a cluster of asteroids located near semimajor axis a = 2.79 AU, has experienced significant dynamical evolution over its lifetime. The family, which was likely created byExpand
Orbital evolution of the Gefion and Adeona asteroid families: close encounters with massive asteroids and the Yarkovsky effect
Abstract Asteroid families are groupings of minor planets identified by clustering in their proper orbital elements; these objects have spectral signatures consistent with an origin in the break-upExpand
Dynamical evolution and chronology of the Hygiea asteroid family
The asteroid (10) Hygiea is the fourth largest asteroid of the main belt, by volume and mass, and it is the largest member of its own family. Previous works investigated the long-term effects ofExpand
The (not so) peculiar case of the Padua family
The Agnia asteroid family was recently studied by Vokrouhlicky et al. because of its peculiar and, so far, unique relationship with the z 1 secular resonance. The Agnia family is almost entirelyExpand
Yarkovsky footprints in the Eos family
Abstract The Eos asteroid family is the third most populous, after Themis and Koronis, and one of the largest non-random groups of asteroids in the main belt. It has been known and studied forExpand
Collisionally Born Family About 87 Sylvia
There are currently more than 1000 multi-opposition objects known in the Cybele population, adjacent and exterior to the asteroid main belt, allowing a more detailed analysis than was previouslyExpand
In search of the source of asteroid (101955) Bennu: Applications of the stochastic YORP model
Abstract Asteroid (101955) Bennu, the target of NASA’s OSIRIS-REx sample return mission, is a D ≈ 0.5  km diameter low albedo near-Earth object. It has a spectral signature consistent with primitiveExpand
A Semianalytical Model for the Motion of the Trojan Asteroids: Proper Elements and Families
In this paper we develop a semianalytical model to describe the long-term motion of Trojan asteroids located in tadpole orbits around the L4 and L5 jovian Lagrangian points. The dynamical model isExpand